Search for galaxy-ICM interaction in rich clusters of galaxies
Search for galaxy-ICM interaction in rich clusters of galaxies
复制标题
在丰富的星系团中寻找星系-ICM 相互作用
DOI：
10.1002/asna.201211879
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发表时间：
2013
影响因子：
0.9
通讯作者：
K.
中科院分区：
文献类型：
--
作者：
Gu;L.; Gandhi;P.; Inada;N.; Kawaharada;M.; Kodama;T.; Konami;S.; Nakazawa;K.; Shimasaku;K.; Xu;Haiguang; Makishima;K.
基于 34 个红移为 0.1-0.9 的松弛丰富星团样本的光学和 X 射线数据，我们研究了两个主要重子含量（星团星系和热等离子体）的相对空间分布。利用 UH88 望远镜拍摄的光度数据，我们使用两种独立的方法（即场背景扣除和色度滤波）确定了每个星团中成员星系的集成径向光剖面。我们样品中每个簇的 ICM 质量分布是使用 XMM-NewtonandChandradata 进行空间分辨光谱分析得出的。当样本被分成红移间隔为 z= 0.11–0.22、0.22–0.45 和 0.45–0.89 的三个子样本时，发现中心 0.65R500 区域的星系光与 ICM 质量比分布从较高红移子样本到较低红移子样本变得陡峭，这意味着星系变得更加集中在 ICM 球体中，朝向较低红移。此外，星系光与总质量比分布也表现出逐渐集中到较低的红移。我们解释说，星系、ICM和暗物质成分在早期阶段（z>0.5）遵循相似的空间分布，而星系相对于ICM和暗物质已经向中心下降。当星系穿过ICM时，这种星系的坠落很可能是由ICM阻力引起的，尽管动态摩擦可以增强最大质量星系的坠落。 （© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA，魏因海姆）
Based on optical and X‐ray data for a sample of 34 relaxed rich clusters with redshift of 0.1–0.9, we studied the relative spatial distribution of the two major baryon contents, the cluster galaxies and the hot plasmas. Using photometric data taken with the UH88 telescope, we determined the integrated radial light profiles of member galaxies in each cluster using two independent approaches, i.e., the field background subtraction and the color‐magnitude filtering. The ICM mass profile of each cluster in our sample was derived from a spatially‐resolved spectral analysis using XMM‐NewtonandChandradata. When the sample is divided into three subsamples with redshift intervals ofz= 0.11–0.22, 0.22–0.45, and 0.45– 0.89, the galaxy light vs. ICM mass ratio profiles for the central 0.65R500regions were found to steepen from the higher‐ to lower‐ redshift subsamples, meaning that the galaxies become more concentrated in the ICM sphere towards lower redshifts. Besides, the galaxy light vs. total mass ratio profiles also exhibit gradual concentration towards lower redshift. We interpret that the galaxies, the ICM, and the dark matter components followed a similar spatial distribution in the early phase (z> 0.5), while the galaxies have fallen towards the center relative to the ICM and dark matter. Such galaxy infall is likely tobe caused by ICM drag when galaxies move through the ICM, even though the dynamical friction can enhance the infall of the most massive galaxies. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)